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Galactic Extinction Curves and Interstellar Dust Models

Galactic Extinction Curves and Interstellar Dust Models. Nozawa, T. and Fukugita, M. (Kavli IPMU, University of Tokyo). 2012/05/08. 1. Introduction. Extinction curve: wavelength-dependence of interstellar extinction by dust

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Galactic Extinction Curves and Interstellar Dust Models

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  1. Galactic Extinction Curves and Interstellar Dust Models Nozawa, T. and Fukugita, M. (Kavli IPMU, University of Tokyo) 2012/05/08

  2. 1. Introduction Extinction curve: wavelength-dependence of interstellar extinction by dust ・ necessary for correcting the SEDs of stars/galaxies ➔ especially, extragalactic objects whose appearances are disturbed by the Galactic interstellar extinction ・ depends on the physical and optical properties of dust ➔ provides information on the composition and size distribution of interstellar dust on the line of sight ➔ holds important clues to the origin and evolution history of interstellar dust

  3. 2. Average interstellar extinction curves in MW Far-UV rise 2175 A bump ➔ small graphite or PAHs B V 〇 CCM relation (Cardelli, Clayton, & Mathis 1989) 　・ Aλ/AV = a(x) + b(x) / RV, where x = 1 / λ 　・ RV : ratio of total-to-selective extinction RV = AV / (AB – AV) cf. RV,ave = 3.05–3.10

  4. 3. Interstellar dust models in MW 　〇 MRNdust model (Mathis, Rumpl, & Nordsieck 1977) 　　・ dust composition : silicate (MgFeSiO4) & graphite (C) 　　・ size distribution : power-law distribution n(a)da ∝a^{-q}da with q=3.5, 0.005 μm ≤ a ≤ 0.25 μm 〇 WD01model (Weingartner & Draine 2001) ・ dust composition : silicate + graphite + PAHs ・ size distribution: power-law with exponential decay + lognormal 0.3 nm ≤ a ≤ 1 μm

  5. 4. Variety of interstellar extinction curves ・ There are a large variety of interstellar extinction curves ・ How much can the properties of interstellar dust change? gray curves: 328 extinction curves derived by Fitzpatrick & Massa (2007) red bars: 1σ ranges including 224 data blue bars: 2σ ranges including 312 data

  6. 5. Comparison to CCM formula and WD curve UV-through-IR extinction curves Close-up of IR extinction curves black: 1σ range of the FM07 data red: CCM curve with Rv = 2.75 blue: CCM curve with Rv = 3.60 green: extinction curve for the case of Rv=3.1 by WD01 fully consistent in UV region Results from CCM formula with Rv = 2.75-3.60 are 0.02-0.06 mag higher than the 1σ range in JHK WD01 model is based on results by Fitzpatrick (1999), which are quite similar to the CCM results

  7. 6. What causes the difference in IR extinction? α = 1.61 α = 1.84 NIR extinction is interpolated by power-law formula Aλ/Av ∝ λ^-α CCM : α= 1.61 from Rieke & Lebofsky (1985) FM07 : α = 1.84 from Martin & Whittet (1990) the value of α is controversial !! α = 1.7 (He et al. 1995) α = 1.8 (Froebrich et al. 2007) α = 2.0 (Nishiyama et al. 2006) α= 2.3 (Larson & Whittet 2005) α = 2.6 (Gosling et al. 2009)

  8. 7.Demonstration of contour plots 1σ range of FM07 data Contour plots for graphite UV UB JHK The 1σ ranges from FM07 data are classified into three groups UV: UV bump (0.22 μm), FUV dip (0.16 μm), FUV rise (0.125 μm) UB: U band and B band JHK: J band, H band, K band A contour plot is depicted for each of the groups defined in the left panel blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band

  9. 8-1. Contour plots for fgra/fsil = 1.0 Case of 1σ data, fgra/fsil = 1.0 Case of 1σ data, fgra/fsil = 1.0 contour plots of amax and q that fulfill the 1σ range of FM07 data for fgra/fsil = 1.0 (Mgra/Msil = 0.78) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band contour plots of amax and q that fulfill the 1σ range of CCM result for fgra/fsil = 1.0 (Mgra/Msil = 0.78) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band

  10. 8-2. Contour plots for fgra/fsil = 0.5 Case of 1σ data, fgra/fsil = 0.5 Case of 1σ data, fgra/fsil = 0.5 contour plots of amax and q that fulfill the 1σ range of FM07 data for fgra/fsil = 0.5 (Mgra/Msil = 0.39) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band contour plots of amax and q that fulfill the 1σ range of CCM result for fgra/fsil = 0.5 (Mgra/Msil = 0.39) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band

  11. 8-3. Contour plots for fgra/fsil = 0.2 Case of 1σ data, fgra/fsil = 0.2 Case of 1σ data, fgra/fsil = 0.2 contour plots of amax and q that fulfill the 1σ range of FM07 data for fgra/fsil = 0.2 (Mgra/Msil = 0.16) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band contour plots of amax and q that fulfill the 1σ range of CCM result for fgra/fsil = 0.2 (Mgra/Msil = 0.16) blue: constraint from UV/FUV green: constraint from UB band red: constraint from JHK band

  12. 9. Summary ・ The extinction ranges in UV regions from FM07 are described by the CCM formula with Rv = 2.75-3.60 ・ The observed range of NIR extinction from FM07 does not match with the results from CCM relation difference : 0.02-0.06 mag ➔ The average interstellar extinction curve is not necessarily universal ・ For the power-law grain-size distribution, 　－ The values of q and amax that satisfy the observed 1σ ranges of FM07 are confined to narrow ranges － There is no combination of q and amax that satisfy the observed ranges when CCM results are adopted

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